We have proven the anisotropy in the angular distribution of the short and intermediate duration GRBs and provided a method for estimating the redshift of the long and bright GRBs by making use only of their gamma ray spectra. Using new statistical methods we confirmed the existence of a separate group of GRBs of intermediate duration. The group delivered evidence that there is a correlation between the early star formation rate and the frequency of the long GRBs. In the proposed research we will carry out multiwavelength (gamma-ray, X-ray and optical) analysis of the Swift and the Fermi data, including the following topics:

- use of discriminant analysis to study dark GRBs

- finding correlations between X-ray and gamma ray data thus connecting the surroundings of the GRB with the central engine

- use of survival analysis to obtain an unbiased distribution of the V visual brightness

- search for subgroups in the GRB samples and elucidate their physical origin

- use of GRBs for cosmology: search for correlations with cosmic matter

- producing light curves from Swift and Fermi (GLAST) data and to build a catalog of redshift corrected lightcurves in the local frames

- search for nanolensing signatures in the lightcurves of GRBs

- search for the hidden jet brakes of the afterglow that can tell us the opening angle of the jet of the GRB. This has not been reassuringly observed in X-rays

most important results
We identified the BATSE's third group also in the BeppoSax, Fermi and Swift datasets. In the Swift data a significant number of the third group GRBs were identified as X-Ray Flashes.
Both the long and intermediate GRBs have the same redshift distributions. The X-ray and optical afterglows are fainter for the intermediate GRBs compared with the long ones: it can be explained by the varying thicknesses of the emitting shells.
In the sky distribution of 283 GRBs with known redshift a strongly significant grouping was found around z=2. The sky distributions of both the BATSE intermediate and short GRBs are significantly non-random.
A new, more efficient background determination was developed for the Fermi satellite - it is based on the satellite's motion.
It was shown that the optical brightness of a GRB depends on the duration, energy and peak-intensity, but does not depend on the X-ray flux and gamma-photon index. This can be connected with the central engine's energy.
For the high-energy spectrum the jet-acceleration was explained by dominant magnetic field. The bright flashes were explained by the synchrotron radiation of photosphere.
The flux and the H column-density are correlated for the afterglows: it suggest either the same physical procedure or a hydrogen-shell ejection before the burst.
For gravitational lensing studies we have shown that only the short Fermi's lightcurves fit for the linear data processing techniques.